The early days of ground-based gamma-ray astronomy in France. Gerard Fontaine - Hillas symposium Heidelberg December

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1 The early days of ground-based gamma-ray astronomy in France Gerard Fontaine - Hillas symposium Heidelberg December

2 Timeline from 1986 to THEMISTOCLE & ASGAT CAT CELESTE Blois 1992 Palaiseau 1992 ICRC + Kruger 1997 Gerard Fontaine - Hillas Symposium Heidelberg December

3 It all started from controversial observations! Claim from EAS experiments (Kiel & Haverah Park) of PeV photons with anomalous muon production - 28 scintillation counters, 1m 2 each - 60,000 showers over 16,775 hours - In the direction of Cygnus X-3 (3,838 hours): excess of 16.6 showers (4.4 σ ) with an angular resolution of 1 + characteristic 4.8 h signal modulation - Very high flux: Φ > 2 PeV = (7.4 ± 3.2) x photons cm -2 s -1 - Muon content similar to hadronic showers... Gerard Fontaine - Hillas Symposium Heidelberg December

4 THEMISTOCLE Concept Tracking High Energy Muons In Showers Triggered On Cherenkov Light Emission - Use gamma beams from cosmic sources to reveal possible new mechanism of photo production at high energies (Cl. Ghesquière). - Cherenkov detection allows a much better angular resolution; - Use the atmosphere as a GigaTon calorimeter => better energy measurement; - Themis site available with 200 heliostats (Ph. Goret ASGAT expt). April 1986: Letter of intent; Dec. 1986: Proposal Gerard Fontaine - Hillas Symposium Heidelberg December

5 Energy Scale aimed at by THEMISTOCLE Gerard Fontaine - Hillas Symposium Heidelberg December

6 Descoping from THEMISTOCLE-300 to THEMISTOCLE-18 Proposal (300 telescopes) Pilot Cherenkov experiment with 18 telescopes approved by IN2P3 in March 1988 Elliptical field 280 x 190 m Gerard Fontaine - Hillas Symposium Heidelberg December

7 THEMISTOCLE-18 Detector Construction from 1988 to 1990 => 80 cm Ø mirror + fast XP2020 PMT + preamp + constant fraction discriminator ns TDC + ADC for each channel Gerard Fontaine - Hillas Symposium Heidelberg December

8 THEMISTOCLE-18 first results (½) Event reconstruction: in the TeV energy range, the light wave front is well described by a cone Laser calibrated timing: a 0.17 ns b 2.7 ns Fitting a 6 parameter cone is highly non-linear. Convergence is slow due to the singularity at the apex and many ridges in the parameter space! Mean time residual: 0.33 ns Ready for science observations in Summer 1990 Gerard Fontaine - Hillas Symposium Heidelberg December

9 THEMISTOCLE-18 first results ( 2 / 2 ) Crab Nebula signal Signal extraction (based on Timing): Distribution of reconstructed directions, u D, u R : Euler angles, local orthonormal coordinate system in mrd. Maximum likelihood method to test the existence of a source signal against the hypothesis of pure background (OFF data). First season on Crab (67 h / winter ): 95 gamma detected at 3.5 σ data on Her X-1 and Cyg X-3: NO signal With additional 95 h ( ) on Crab: 282±54 gamma at 6 σ, with an angular resolution of 2.2 mrad (0.13 ). ( ICHEP Dallas Feb 1992, XIII Physics in Collision Heidelberg 1993 ) Gerard Fontaine - Hillas Symposium Heidelberg December

10 THEMISTOCLE energy mesurement & hadron rejection Energy estimation and spectrum: - The amplitudes of the signals from a shower are used in a global fit of the radial density distributions predicted by MC generation of gamma showers at different energies. - In addition to the energy estimate, the quality of this fit provides a discrimination between gamma rays (good fit) and hadrons (bad fit). - The energy scale is set by fitting the trigger rate (dominated by hadronic showers). Publication in Astropart. Phys (1993) done with pure proton background has a biased energy scale! The threshold is NOT 3 TeV as stated Crab Nebula Integral Spectrum Roma ICRC paper (1995), with a more realistic background taking into account He and heavier ions. A total of 388 h of Crab data => 407±68 gamma E > 2 TeV detected at 6.6 σ, with spectrum extending from 2 to 13 TeV. 22 publications in conference proceedings over 8 years, but only one in a referred journal! Gerard Fontaine - Hillas Symposium Heidelberg December

11 THEMISTOCLE lessons learned On the technical side - Wavefront sampling can be used for gamma-ray astronomy; - Good reconstruction (direction and energy) requires a minimum of 12 samples for each shower; - 18 telescopes was a bit too low in this respect and an array of 40 would have been much more efficient. On the scientific side - Confirmation that TeV gamma rays are emitted in the Universe; - But their fluxes are much lower than anticipated and no emission is seen from Her X-1 and Cyg X-3; - No hope for a discovery of a new mechanism of photo production at high energies, while at the same time the first results of the HERA collider were showing a conventional γ-p interaction up to 200 GeV CM energy. Observations (almost) stopped in 1995 But a strong interest in gamma-ray sources had been triggered, and was going to continue Gerard Fontaine - Hillas Symposium Heidelberg December

12 Gamma-ray astronomy status in 1992 Gamma-ray emission of the Crab Nebula had already been discovered by the Whipple Obs. group (Ap J 1989) (Thanks to T. Weekes tenacity and to A.M. Hillas analysis method) A.E Chudakov s worries and satisfaction at the Blois conference on Particle Astrophysics (1992): Gerard Fontaine - Hillas Symposium Heidelberg December

13 Towards a Major Atmospheric Cherenkov Detector A Dream not yet true in 1992! And a wink to a concept of hybrid array with 54 Small sized, Medium sized and 3-7 Large sized telescopes Gerard Fontaine - Hillas Symposium Heidelberg December (G.F.)

14 The CAT Project After the 13 th ECRS conference in Geneva (1992) and the announcement of the HEGRA Cherenkov project : the CAT imaging telescope was proposed in 1993 by B. Degrange et al for the Themis site: - Imaging technique (following A.M. Hillas pioneering work) - Modest mirror size (16 m 2 ) - Very fast and fine grained camera (546 pixels 0.12 in Ø) - Advanced analysis techniques based on image matching with a library of precomputed shapes. First light in 1996: Despite a much smaller mirror size (16 m 2 ) than that of Whipple (75 m 2 ), fine grained imaging made it possible for CAT to reach a similar sensitivity and energy threshold (250 GeV)! Gerard Fontaine - Hillas Symposium Heidelberg December

15 CAT Telescope and Camera Gerard Fontaine - Hillas Symposium Heidelberg December

16 CAT Results and Timeline Dec. 1992: Letter of Intent July 1993: Proposal 1994: Approved by IN2P3 1996: First light - Nov. 1998: «The CAT imaging telescope» NIM, vol. A 416, pp Nov. 1998: «A new analysis method» NIM, vol. A 416, pp Oct. 1999: «VHE Mkn 501 in 1997» A&A, vol. 350, pp Aug. 2001: «Temporal Mkn 421» A&A, vol. 374, pp Aug. 2002: «Detect. 1ES » A&A, vol. 391 (2002), pp L25-L : End of observations + 31 publications in conference proceedings over 9 years : End of the experiment incl. 1ES (& 1ES ) at Meudon 2003 Gerard Fontaine - Hillas Symposium Heidelberg December

17 April 1997: An important Milestone Simultaneous observation of the Mrk 501 flare by Whipple, HEGRA and CAT Reported at the 25th ICRC in Durban and the Kruger Workshop (1997) Gerard Fontaine - Hillas Symposium Heidelberg December

18 Revisiting wave-front sampling Scientific need to bridge the energy gap [10 GeV 250 GeV] between space-borne and ground-based observations Cherenkov technique below 100 GeV requires very large mirrors Opportunity to use again the Themis solar plant array! 200 heliostats (54 m2 each) concentrating the sun s power at the top of a 100 m height tower. Gerard Fontaine - Hillas Symposium Heidelberg December

19 The CELESTE project Wave-front sampling detector approved in 1996 as a multi-step project (6 -> 18 > 40 mirrors 2000 m 2 ) led by E. Paré Required secondary optics on top of the tower 1 GHz FADCs First light in 1998 Gerard Fontaine - Hillas Symposium Heidelberg December

20 CELESTE results Sensitivity down to 30 GeV 1998: «Prototype tests» NIM, vol. A 412, pp : «CELESTE: an atmospheric» NIM, vol. A 490, pp Feb. 2002: «Measurement Crab 60 GeV» ApJ 566, pp : «Mrk 421, Mrk 501 and 1ES GeV» A&A 459, Crab nebula gamma-ray spectrum Gerard Fontaine - Hillas Symposium Heidelberg December

21 Moral of the story Difficulties with the CELESTE solar farm approach: Shape of the wave-front (conical above 1 TeV, but spherical around 100 GeV) Limited field of view ( 1 defined by the size of the secondary optics) Albedo and weather issues Better move to another site and Go for imaging! Thanks again to A.M. Hillas Combining : - Large dish as in Whipple, - Stereoscopy as in HEGRA - Fast and fine grained camera(s) + advanced analysis techniques as in CAT - With a field of view as large as possible. Gerard Fontaine - Hillas Symposium Heidelberg December

22 And then came the H.E.S.S. era Thank you Any questions? Gerard Fontaine - Hillas Symposium Heidelberg December

23 Backup slides Gerard Fontaine - Hillas Symposium Heidelberg December

24 Measurement of the Crab Nebula Spectrum ASGAT 0.6 TeV THEMISTOCLE [2 13 TeV] Crab Nebula Integral Spectrum Gerard Fontaine - Hillas Symposium Heidelberg December

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